Astronomy and Astrophysics – Astronomy
Scientific paper
May 1993
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1993pasp..105..468l&link_type=abstract
Astronomical Society of the Pacific, Publications (ISSN 0004-6280), vol. 105, no. 687, p. 468-475.
Astronomy and Astrophysics
Astronomy
33
Abundance, Boron, Dwarf Stars, F Stars, Stellar Composition, Stellar Spectra, Astronomical Spectroscopy, Beryllium, Galactic Halos, Hubble Space Telescope, Lithium, Spaceborne Astronomy
Scientific paper
The B I 2496.8 A resonance line and HST/GHRS echelle spectra are used with model atmospheres and synthetic spectra to derive the B abundance of the F dwarfs Procyon (Alpha Canis Minoris), Theta Ursae Majoris, and Iota Pegasi. The B abundance of Theta UMa and Iota Peg is similar to that derived by Boesgaard and Heacox (1978) from the B II resonance line in spectra of A- and B-type stars. These two dwarfs show normal abundances of Li, Be, and B. Procyon, which is highly depleted in Li and Be, is depleted in B by a factor of at least 3. Comparison of the spectra of Procyon and the halo dwarf HD 140283 shows that the B abundance assigned by Duncan et al. (1992) to three halo dwarfs is not greatly overestimated as a result of contamination of the B I line by an unidentified line.
Edvardsson Bengt
Lambert David L.
Lemke Michael
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